The Wing three color system consists of narrow and
intermediate band interference filters centered on the TiO
bandhead at 719 nm, and on two relatively line-free spectral
regions at 754 nm and 1024 nm. A TiO-index is formed from
the photometry; this index measures the relative strength of
TiO feature. The TiO absorption strength is very
sensitive to temperature for cool stars and is expected to
be strong in the cooler star spot regions with T < 4200 K.
TiO photometry has an advantage over conventional
photometry in that it provides unambiguous measures of the
fractional cool starspot coverage. As the stars rotate, the
variation in the TiO index yields information about the
longitudinal distribution of the starspots. Importantly,
combining the TiO curves with the V-band and near-IR light
curves allows the discrimination of white-light plage and
cool starspot contributions. Initial results indicate that
the observed V-band light variations found for \lambda And
and IM Peg primarily arise from bright-spot (plage) features
rather than dark starspots as is usually assumed. In the
shorter period, classical RS CVn stars V711 Tau and II Peg,
the continuum light curves appear to be dominated by dark
spots. Models using both bright and dark spot features have
been developed and being used to analyzed the light and
TiO-index curves. The models account for the cool/hot spot
characteristics such as fill-factor, longitude, latitude,
and temperatures. We will discuss the results of the
modeling for these stars and the implications for stellar
dynamo theories.

This research is supported by NSF/RUI grant AST 00-71260 and
an AAS Small Research Grant which we gratefully acknowledge.